COVER INFORMATION Station: URUMQI (Code Ur ) Experiment: Network Monitoring Experiment Exp. Code: N21L2 Schedule Version: 1.00 Processed by SCHED version: 11.60 Release 11.6; April 2020 PI: Benito Marcote Address: JIVE Oude Hoogeveensedijk 4 7991PD Dwingeloo The Netherlands Phone: +31 521 596 508 EMAIL: marcote@jive.eu Fax: Phone during observation: +31 521 596 508 Observing mode: Notes: 18cm NME and ftp fringe test for Session 2 2021 (1024 Mbps, L+R, 2-bit sampling, 32 MHz filters) Please send the disk pack by express to JIVE COVER LETTER: This is the schedule for the 18cm NME and ftp fringe-test on 27 May 2021 involving the following antennas: Jb1, Wb, Ef, Mc, Nt, On85, T6, Ur, Tr, Hh, Sv, Zc, Bd, Ir, Sr, Cm, Da, De, Kn, Pi. The NME uses a standard setup with 1024 Mbps. The schedule consists of long integrations on calibrators J0956+2515. The following ftp-fringe tests are scheduled throughout the experiment (UT times): 12:10:00 (scan 2, 2 sec, J0956+2515) 12:40:00 (scan 4, 2 sec, J0956+2515) 13:10:00 (scan 6, 2 sec, J0956+2515) 13:40:00 (scan 8, 2 sec, J0956+2515) 14:10:00 (scan 10, 2 sec, J0956+2515) 14:40:00 (scan 12, 2 sec, J0956+2515) Good luck with the session! Benito Marcote Mattermost: coms.evlbi.org Schedule for URUMQI (Code Ur ) Page 2 Network Monitoring Experiment UP: D => Below limits; H => Below horizon mask; W => still slewing at end; blank => Up. Early: Seconds between end of slew and start. Dwell: On source seconds. Disk: GBytes recorded to this point. TPStart: Recording start time. Frequencies are LO sum (band edge). SYNC: Time correlator is expected to sync up. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Disk TPStart Stop UT LST EL AZ HA UP ParA Dwell GBytes SYNC ---------------------------------------------------------------------------------------- --- Thu 27 May 2021 Day 147 --- Next scan frequencies: 1626.49 1626.49 1626.49 1626.49 1690.49 1690.49 1690.49 1690.49 Next BBC frequencies: 326.49 326.49 326.49 326.49 390.49 390.49 390.49 390.49 Next scan bandwidths: 32.00 32.00 32.00 32.00 32.00 32.00 32.00 32.00 12 00 00 J0956+2515 10 09 47 71.5 188.4 0.2 6.7 0 0 12 00 00 12 02 00 =OK290 10 11 47 71.5 189.8 0.2 7.9 120 15 12 00 01 12 07 00 J0956+2515 10 16 48 71.3 193.3 0.3 10.7 297 15 12 07 00 12 12 00 =OK290 10 21 49 71.0 196.8 0.4 13.4 300 54 12 07 01 12 15 00 J0956+2515 10 24 49 70.9 198.8 0.4 15.0 177 54 12 15 00 12 27 00 =OK290 10 36 51 70.0 206.6 0.6 21.0 720 146 12 15 01 12 30 00 J0956+2515 10 39 52 69.8 208.4 0.7 22.4 177 146 12 30 00 12 42 00 =OK290 10 51 54 68.6 215.4 0.9 27.6 720 238 12 30 01 12 45 00 J0956+2515 10 54 54 68.3 217.0 0.9 28.8 177 238 12 45 00 12 57 00 =OK290 11 06 56 66.9 223.1 1.1 33.2 720 331 12 45 01 13 00 00 J0956+2515 11 09 56 66.5 224.5 1.2 34.2 178 331 13 00 00 13 12 00 =OK290 11 21 58 64.9 229.9 1.4 37.8 720 423 13 00 01 13 15 00 J0956+2515 11 24 59 64.5 231.2 1.4 38.6 178 423 13 15 00 13 27 00 =OK290 11 37 01 62.7 235.8 1.6 41.6 720 515 13 15 01 13 30 00 J0956+2515 11 40 01 62.3 236.9 1.7 42.2 178 515 13 30 00 13 42 00 =OK290 11 52 03 60.4 241.1 1.9 44.6 720 608 13 30 01 13 45 00 J0956+2515 11 55 04 59.9 242.0 2.0 45.1 178 608 13 45 00 13 57 00 =OK290 12 07 06 58.0 245.7 2.2 47.0 720 700 13 45 01 14 00 00 J0956+2515 12 10 06 57.5 246.6 2.2 47.4 178 700 14 00 00 14 12 00 =OK290 12 22 08 55.5 249.9 2.4 48.8 720 792 14 00 01 14 15 00 J0956+2515 12 25 09 54.9 250.7 2.5 49.2 178 792 14 15 00 14 27 00 =OK290 12 37 11 52.9 253.6 2.7 50.3 720 885 14 15 01 14 30 00 J0956+2515 12 40 11 52.3 254.4 2.7 50.5 178 885 14 30 00 14 42 00 =OK290 12 52 13 50.2 257.1 2.9 51.4 720 977 14 30 01 14 45 00 J0956+2515 12 55 14 49.7 257.8 3.0 51.6 178 977 14 45 00 14 57 00 =OK290 13 07 16 47.5 260.3 3.2 52.2 720 1069 14 45 01 14 58 00 J0956+2515 13 08 16 47.4 260.5 3.2 52.3 58 1069 14 58 00 15 00 00 =OK290 13 10 16 47.0 260.9 3.2 52.3 120 1085 14 58 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: sess221.L1024 --- WARNING --- This group does not match an entry in the frequency catalog. This might be ok because the catalog is not complete. But be very careful to be sure that the setup is correct. Setup group: 14 Station: URUMQI Total bit rate: 1024 Format: MARK5B Bits per sample: 2 Sample rate: 64.000 Number of channels: 8 DBE type: DBBC_DDC Speedup factor: 1.00 Disk used to record data. 1st LO= 1300.00 1300.00 1300.00 1300.00 1300.00 1300.00 1300.00 1300.00 Net SB= L L U U L L U U IF SB = U U U U U U U U Pol. = RCP LCP RCP LCP RCP LCP RCP LCP BBC = 1 9 1 9 2 10 2 10 BBC SB= L L U U L L U U IF = A2 C1 A2 C1 A2 C1 A2 C1 The following frequency sets based on these setups were used. Frequency Set: 8 Setup file default. Used with PCAL = off LO sum= 1626.49 1626.49 1626.49 1626.49 1690.49 1690.49 1690.49 1690.49 BBC fr= 326.49 326.49 326.49 326.49 390.49 390.49 390.49 390.49 Bandwd= 32.00 32.00 32.00 32.00 32.00 32.00 32.00 32.00 Matching frequency sets: 8 Track assignments are: track1= 10, 14, 2, 6, 12, 16, 4, 8 barrel=roll_off POSITIONS OF SOURCES USED IN RECORDING SCANS Source Source position (RA/Dec) Error (B1950) (J2000) (Date) (mas) OK290 09 53 59.738482 * 09 56 49.875376 09 58 01.250003 0.41 * J0956+2515 25 29 33.58581 * 25 15 16.04991 25 09 19.59708 0.37 0953+254 /home/guest/rmc/SCHED/sched11.6/catalogs/sources.gsfc J0956+25 GSFC 2016a X/S astro solution, 26975 observations. SOURCE SCAN SUMMARY FOR SOURCES LISTED ABOVE Scan hours are for recording scans only. Baseline hours are only counted for scans above horizon at both ends. Source Setup file Frequency sets Observing hours (duplicates not shown) Scan Baseline J0956+2515 sess221.L1024 1 2 3 4 5 6 7 8 9 10 11 14 + 2.350 446.500 EFFECT OF SOLAR CORONA The solar corona can cause unstable phases for sources too close to the Sun. SCHED provides warnings at individual scans for distances less than 10 degrees. The distance from the Sun to each source in this schedule is: Source Sun distance (deg) J0956+2515 76.7 Barry Clark estimates from predictions by Ketan Desai of IPM scattering sizes that the Sun will cause amplitude reductions on the longest VLBA baselines at a solar distance of 60deg F^(-0.6) where F is in GHz. For common VLBI bands, this is: 327 MHz 117. deg 610 MHz 81. deg 1.6 GHz 45. deg 2.3 GHz 36. deg 5.0 GHz 23. deg 8.4 GHz 17. deg 15.0 GHz 12. deg 22.0 GHz 9. deg 43.0 GHz 6. deg